高红移半导体宽带光偏振测量中各向异性双约束Lorentz不变性和CPT破坏的改进约束
Improved Constraints on Anisotropic Birefringent Lorentz Invariance and CPT Violation from Broadband Optical Polarimetry of High Redshift Galaxies
摘要：
在标准模型扩展（SME）的框架下，利用宽带光学偏振技术对活动星系核和伽马射线暴余辉等高红移天体源的宇宙真空双折射信号进行了研究，提出了改进的各向异性洛伦兹不变性和电荷-宇称-时间（CPT）破坏的约束条件.我们将Kislat 2018中的工作推广到CPT-偶数和CPT-奇数情况下的任意质量维度，该工作研究了SME质量维度$d = 4$情况。然后，我们分别对维度$d = 4$、$d = 5$和$d = 6$模型的所有10、16和42个各向异性双折射SME系数提出约束，使用天空上1278个唯一源的奇数d的7554个观测值和偶数d的7376个观测值，据我们所知，包括迄今为止文献中最完整的河外星系源光学偏振目录。与Kislat 2018和Kislat和Krawczynski 2017中分析的44和45个宽带光学偏振测量观测的较小样本相比，我们的维度$d = 4$和$d = 5$平均约束的灵敏度分别为35和10倍，对应于这些研究的允许SME参数空间体积分别减少了15和16个数量级。使用分光偏振法，来自个体视线的约束可以显著更强。尽管如此，由于我们目录中观测和视线数量的增加，我们的平均$d = 4$和$d = 5$宽带约束分别在Kislat 2018和Kislat和Krawczynski 2017使用独立数据集和改进的分析方法使用分光偏振法的2和12倍范围内。相比之下，我们的所有42个双折射SME系数的各向异性约束$d = 6$是第一次在文献中提出。
英文摘要：
In the framework of the Standard Model Extension (SME), we present improved constraints on anisotropic Lorentz invariance and Charge-Parity-Time (CPT) violation by searching for astrophysical signals of cosmic vacuum birefringence with broadband optical polarimetry of high redshift astronomical sources, including Active Galactic Nuclei and Gamma-Ray Burst afterglows. We generalize the work in Kislat 2018, which studied the SME mass dimension $d = 4$ case, to arbitrary mass dimension for both the CPT-even and CPT-odd cases. We then present constraints on all 10, 16, and 42 anisotropic birefringent SME coefficients for dimension $d = 4$, $d = 5$, and $d = 6$ models, respectively, using 7554 observations for odd d and 7376 observations for even d of 1278 unique sources on the sky, which, to our knowledge, comprises the most complete catalog of optical polarization from extragalactic sources in the literature to date. Compared to the smaller sample of 44 and 45 broadband optical polarimetry observations analyzed in Kislat 2018 and Kislat and Krawczynski 2017, our dimension $d = 4$ and $d = 5$ average constraints are more sensitive by factors of 35 and 10, corresponding to a reduction in allowed SME parameter space volume for these studies of 15 and 16 orders of magnitude, respectively. Constraints from individual lines of sight can be significantly stronger using spectropolarimetry. Nevertheless, due to the increased number of observations and lines of sight in our catalog, our average $d = 4$ and $d = 5$ broadband constraints are within factors of 2 and 12 of previous constraints using spectropolarimetry from Kislat 2018 and Kislat and Krawczynski 2017, respectively, using an independent data set and an improved analysis method. By contrast, our anisotropic constraints on all 42 birefringent SME coefficients for $d = 6$ are the first to be presented in the literature.
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